Abstract
Modeled searches of gravitational wave signals from compact binary mergers rely on template waveforms determined by the theory of general relativity (GR). Once a signal is detected, one generally performs the model agnostic test of GR, either looking for consistency between the GR waveform and data or introducing phenomenological deviations to detect the departure from GR. The nontrivial presence of beyond-GR physics can alter the waveform and could be missed by the GR template-based searches. A recent study [H. Narola, Beyond general relativity: Designing a template-based search for exotic gravitational wave signals, Phys. Rev. D 107, 024017 (2023)PRVDAQ2470-001010.1103/PhysRevD.107.024017] targeted the binary black hole merger, assuming the parametrized deviation in lower post-Newtonian terms, and demonstrated a mild effect on the search sensitivity. Surprisingly, for the search space of binary neutron star (BNS) systems where component masses range from 1 to 2.4M⊙ and parametrized deviations span 1σ width of the deviation parameters measured from the GW170817 event, the GR template bank is highly ineffectual for detecting the non-GR signals. Here, we present a new hybrid method to construct a non-GR template bank for the BNS search space. The hybrid method uses the geometric approach of three-dimensional lattice placement to cover most of the parameter space volume, followed by the random method to cover the boundary regions of parameter space. We find that the non-GR bank size is ∼15 times larger than the conventional GR bank and is effectual toward detecting non-GR signals in the target search space.
| Original language | English |
|---|---|
| Article number | 124049 |
| Number of pages | 16 |
| Journal | Physical Review D |
| Volume | 109 |
| Issue number | 12 |
| DOIs | |
| Publication status | Published - 15 Jun 2024 |
Bibliographical note
Publisher Copyright:© 2024 American Physical Society.
Funding
We thank Ian Harry for carefully reading the manuscript and for offering several comments and suggestions to improve the presentation and content of the paper. We are highly grateful for the suggestions received from Alex Nielsen, Tito Dal Canton, and Thomas Dent. A. S. thanks IIT Gandhinagar for the research fellowship. S. R. was supported by the research program of the Netherlands Organization for Scientific Research (NWO) . We acknowledge computational resources provided by IIT Gandhinagar and also thank high performance computing support staff at IIT Gandhinagar for their help and cooperation. We gratefully acknowledge computational resources provided by the LIGO Laboratory and supported by the NSF Grants No. PHY-0757058 and No. PHY-0823459. This research has made use of data, software and/or web tools obtained from the Gravitational Wave Open Science Center, a service of LIGO Laboratory [84] , the LIGO Scientific Collaboration, and the Virgo Collaboration. The material of this paper is based upon work supported by NSF ' s LIGO Laboratory, which is a major facility fully funded by the National Science Foundation. To obtain the waveforms and PN coefficients, we use the LAL SIMULATION package of the LIGO Algorithms Library (LAL) software suite [85] . The fitting factor studies were performed by modifying pycbc_banksim code implemented in the P Y CBC library [86] . Our analysis utilizes NumPy [87] , SciPy [80] , and Matplotlib [88] .
| Funders | Funder number |
|---|---|
| Nederlandse Organisatie voor Wetenschappelijk Onderzoek | |
| National Science Foundation | PHY-0823459, PHY-0757058 |